Properties of Extremely Asymmetric Magnetic Reconnection
The behavior of extremely asymmetric magnetic reconnections is numerically investigated. The asymmetry is defined as the ratio k of the magnetic fields on both sides of the isothermal initial current sheet. This work is an extension of our previous research for 1 < k ≤ 2 to further asymmetry 2 &l...
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Veröffentlicht in: | The Astrophysical journal 2019-02, Vol.872 (2), p.147 |
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description | The behavior of extremely asymmetric magnetic reconnections is numerically investigated. The asymmetry is defined as the ratio k of the magnetic fields on both sides of the isothermal initial current sheet. This work is an extension of our previous research for 1 < k ≤ 2 to further asymmetry 2 < k ≤ 20. In our previous work, Nitta et al., we clarified that even for a slight asymmetry k ≤ 2, the reconnection structure drastically changes from symmetric standard models like the Petschek model. The properties of the asymmetric system are a (1) two-layered non-uniform reconnection jet, (2) contact discontinuity (CD) in the lower beta side (LBS) plasmoid between the plasmas coming from both sides of the current sheet, and (3) forward fast shock (FFS) in front of the higher beta side (HBS) plasmoid. We aim to clarify, in this paper, how these properties change and whether new aspects appear for further asymmetric cases. We have confirmed that, even under strongly asymmetric circumstances, the CD in the LBS plasmoid and the two-layered jet structure hold; however, the FFS disappears for extremely asymmetric cases. The fraction of the HBS plasma component increases in the reconnection outflow as k increases. The reconnection rate decreases as a power-law function of k. |
doi_str_mv | 10.3847/1538-4357/aade98 |
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The asymmetry is defined as the ratio k of the magnetic fields on both sides of the isothermal initial current sheet. This work is an extension of our previous research for 1 < k ≤ 2 to further asymmetry 2 < k ≤ 20. In our previous work, Nitta et al., we clarified that even for a slight asymmetry k ≤ 2, the reconnection structure drastically changes from symmetric standard models like the Petschek model. The properties of the asymmetric system are a (1) two-layered non-uniform reconnection jet, (2) contact discontinuity (CD) in the lower beta side (LBS) plasmoid between the plasmas coming from both sides of the current sheet, and (3) forward fast shock (FFS) in front of the higher beta side (HBS) plasmoid. We aim to clarify, in this paper, how these properties change and whether new aspects appear for further asymmetric cases. We have confirmed that, even under strongly asymmetric circumstances, the CD in the LBS plasmoid and the two-layered jet structure hold; however, the FFS disappears for extremely asymmetric cases. The fraction of the HBS plasma component increases in the reconnection outflow as k increases. The reconnection rate decreases as a power-law function of k.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aade98</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Asymmetry ; Current sheets ; Earth ; ISM: magnetic fields ; Magnetic fields ; Magnetic properties ; Magnetic reconnection ; magnetohydrodynamics (MHD) ; Plasmas (physics) ; Power law ; Sun: flares</subject><ispartof>The Astrophysical journal, 2019-02, Vol.872 (2), p.147</ispartof><rights>2019. The American Astronomical Society. 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J</addtitle><description>The behavior of extremely asymmetric magnetic reconnections is numerically investigated. The asymmetry is defined as the ratio k of the magnetic fields on both sides of the isothermal initial current sheet. This work is an extension of our previous research for 1 < k ≤ 2 to further asymmetry 2 < k ≤ 20. In our previous work, Nitta et al., we clarified that even for a slight asymmetry k ≤ 2, the reconnection structure drastically changes from symmetric standard models like the Petschek model. The properties of the asymmetric system are a (1) two-layered non-uniform reconnection jet, (2) contact discontinuity (CD) in the lower beta side (LBS) plasmoid between the plasmas coming from both sides of the current sheet, and (3) forward fast shock (FFS) in front of the higher beta side (HBS) plasmoid. We aim to clarify, in this paper, how these properties change and whether new aspects appear for further asymmetric cases. We have confirmed that, even under strongly asymmetric circumstances, the CD in the LBS plasmoid and the two-layered jet structure hold; however, the FFS disappears for extremely asymmetric cases. The fraction of the HBS plasma component increases in the reconnection outflow as k increases. The reconnection rate decreases as a power-law function of k.</description><subject>Astrophysics</subject><subject>Asymmetry</subject><subject>Current sheets</subject><subject>Earth</subject><subject>ISM: magnetic fields</subject><subject>Magnetic fields</subject><subject>Magnetic properties</subject><subject>Magnetic reconnection</subject><subject>magnetohydrodynamics (MHD)</subject><subject>Plasmas (physics)</subject><subject>Power law</subject><subject>Sun: flares</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNp9kEtLxDAUhYMoOI7uXRbEnXXyaF7LYRgfMKKIgruQJql0mDY1yYD997ZUdCOu7oNzzr18AJwjeE1EwReIEpEXhPKF1tZJcQBmP6tDMIMQFjkj_O0YnMS4HUcs5QyIp-A7F1LtYuarbP2Zgmvcrs-WsW8al0Jtsgf93ro0NM_O-LZ1JtW-PQVHld5Fd_Zd5-D1Zv2yuss3j7f3q-UmNwUuUs4Eq0qJpCAIFlBzzLi03GKsWcElFdJww4iBlvLSaiYowaUViAuOpaMlJHNwMeV2wX_sXUxq6_ehHU4qTBgVHFGBBxWcVCb4GIOrVBfqRodeIahGPmqEoUYYauIzWK4mS-2738x_5Jd_yHW3VcOrCis0mDpbkS8s_XJh</recordid><startdate>20190220</startdate><enddate>20190220</enddate><creator>Nitta, S.</creator><creator>Kondoh, K.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0001-9838-7765</orcidid></search><sort><creationdate>20190220</creationdate><title>Properties of Extremely Asymmetric Magnetic Reconnection</title><author>Nitta, S. ; Kondoh, K.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c424t-686fb919831040a72679d7d22a6479589c7c63c0d57bda68532bd8178729e5b03</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Astrophysics</topic><topic>Asymmetry</topic><topic>Current sheets</topic><topic>Earth</topic><topic>ISM: magnetic fields</topic><topic>Magnetic fields</topic><topic>Magnetic properties</topic><topic>Magnetic reconnection</topic><topic>magnetohydrodynamics (MHD)</topic><topic>Plasmas (physics)</topic><topic>Power law</topic><topic>Sun: flares</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Nitta, S.</creatorcontrib><creatorcontrib>Kondoh, K.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Nitta, S.</au><au>Kondoh, K.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Properties of Extremely Asymmetric Magnetic Reconnection</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2019-02-20</date><risdate>2019</risdate><volume>872</volume><issue>2</issue><spage>147</spage><pages>147-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>The behavior of extremely asymmetric magnetic reconnections is numerically investigated. The asymmetry is defined as the ratio k of the magnetic fields on both sides of the isothermal initial current sheet. This work is an extension of our previous research for 1 < k ≤ 2 to further asymmetry 2 < k ≤ 20. In our previous work, Nitta et al., we clarified that even for a slight asymmetry k ≤ 2, the reconnection structure drastically changes from symmetric standard models like the Petschek model. The properties of the asymmetric system are a (1) two-layered non-uniform reconnection jet, (2) contact discontinuity (CD) in the lower beta side (LBS) plasmoid between the plasmas coming from both sides of the current sheet, and (3) forward fast shock (FFS) in front of the higher beta side (HBS) plasmoid. We aim to clarify, in this paper, how these properties change and whether new aspects appear for further asymmetric cases. We have confirmed that, even under strongly asymmetric circumstances, the CD in the LBS plasmoid and the two-layered jet structure hold; however, the FFS disappears for extremely asymmetric cases. The fraction of the HBS plasma component increases in the reconnection outflow as k increases. The reconnection rate decreases as a power-law function of k.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/aade98</doi><tpages>17</tpages><orcidid>https://orcid.org/0000-0001-9838-7765</orcidid><oa>free_for_read</oa></addata></record> |
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subjects | Astrophysics Asymmetry Current sheets Earth ISM: magnetic fields Magnetic fields Magnetic properties Magnetic reconnection magnetohydrodynamics (MHD) Plasmas (physics) Power law Sun: flares |
title | Properties of Extremely Asymmetric Magnetic Reconnection |
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